High-Precision Distance Measurements with Classical Pulsating Stars

J. Astrophys. Astr. (0000) 000: #### DOI High-precision distance measurements with classical pulsating stars Anupam Bhardwaj1 1Kavli Institute for Astronomy and Astrophysics, Peking University, Yi He Yuan Lu 5, Hai Dian District, Beijing 100871, China. *Corresponding author. E-mail: [email protected] MS received 21 Jun 2020; accepted 29 Jun 2020. In original form 12 May 2020. Abstract. Classical Cepheid and RR Lyrae variables are radially pulsating stars that trace young and old-age stellar populations, respectively. These classical pulsating stars are the most sensitive probes for the precision stellar astrophysics and the extragalactic distance measurements. Despite their extensive use as standard candles thanks to their well-defined Period-Luminosity relations, distance measurements based on these objects suffer from their absolute primary calibrations, metallicity effects, and other systematic uncertainties. Here, I present a review of classical Cepheid, RR Lyrae, and type II Cepheid variables starting with a historical introduction and describing their basic evolutionary and pulsational properties. I will focus on recent theoretical and observational efforts to establish absolute scale for these standard candles at multiple wavelengths. The application of these classical pulsating stars to high-precision cosmic distance scale will be discussed along with observational systematics. I will summarize with an outlook for further improvements in our understanding of these classical pulsators in the upcoming era of extremely large telescopes. Keywords. Stars: Variables: Cepheids, RR Lyrae, Type II Cepheids, Stars: evolution, Stars: oscillations, Cos- mology: distance scale 1. Introduction by Wilhelmina Flemming and reported in Pickering (1889). Following this discovery, Solon Bailey initi- Stars are primary engines of cosmic evolution and play ated a search for variable stars in the GGCs from the a crucial role in our understanding of the Universe. Harvard College Observatory in 1893 and discovered Variable stars, in particular, provide information about hundreds of “cluster variables”. Bailey later separated the stellar properties including physical parameters, in- the cluster variables as RR Lyrae subtypes but the RR ternal and external envelope structure and composition, Lyrae itself was discovered by Wilhelmina Flemming and probe both the stellar evolution and cosmic dis- (Pickering et al., 1901). Historically, W Virginis was tances. The first variable star was discovered more than the prototype of Type II Cepheids (T2Cs) and it was four centuries back in 1596 by David Fabricius which discovered by Schönfeld (1866). The short-period rep- was later named as Omicron Ceti or Mira and now rep- resentative of T2Cs, BL Herculis was discovered by resents one of the subclasses belonging to the long- Hoffmeister (1929) and the variability of long-period 1 arXiv:2006.16262v1 [astro-ph.SR] 29 Jun 2020 period variables. The short-period, typically fainter, RV Tauri was first observed by Ceraski (1905) . A variable stars were not well-known until two British as- more detailed historical overview of classical Cepheids, tronomers, Edward Pigott and John Goodricke started RR Lyrae and T2Cs can be found in Catelan & Smith observations of β Persei (Algol) in 1782 (Goodricke, (2015) but this brief introduction demonstrates that the 1783). A few years later, Pigott detected the variability Cepheid and RR Lyrae stars represent two of the oldest in η Aquilae, the first known Cepheid variable. At the and therefore well-studied subtypes of variable stars. same time, Goodricke discovered δ Cephei (Goodricke, The observations of Cepheids in the Magellanic 1786), which represents classical Cepheid variables as Clouds (Leavitt, 1908) led to the discovery of a re- one of the most important classes of pulsating variables lation between their pulsation period and luminosity in the modern astronomy. (Leavitt & Pickering, 1912). This relation is commonly About a century later the first variable stars within a Galactic globular cluster (GGC) were discovered 1https://www.aavso.org c Indian Academy of Sciences 1 #### Page 2 of 1 J. Astrophys. Astr. (0000) 000: #### known as “Cepheid Period-Luminosity relation (PLR)” or the Leavitt Law honouring the discoverer. Ever since, classical Cepheids have played a fundamental role in the extragalactic distance measurements. Ed- win Hubble used Cepheid PLR to determine reliable distance to the M31 and discovered that Andromeda, assumed to be a gaseous nebula at that time, is another galaxy beyond our Milky Way (Hubble, 1926). Cepheid-based distances to the galaxies as far as the Virgo cluster allowed Hubble to discover a linear cor- relation between the apparent distances to galaxies and their recessional velocities (Hubble, 1929) - the more distant the galaxy, the faster it moves away from us - now known as the Hubble-Lemaˆıtre law, providing the first evidence of the expanding universe. The slope of the velocity over distance is the Hubble constant (H0), which parameterizes the current expansion rate of the Universe. The current H0 values in the late evolutionary universe are in tension with early universe measurements (Riess et al., 2018a; Planck Collaboration et al., 2018) and therefore understanding the systematics in- volved in standard candles is critical to resolve the H 0 Figure 1. Hertzsprung-Russell diagram displaying schematic tension, and improve the precision of cosmic distance representation of classical pulsating variable stars. A mod- scale. On the other hand, RR Lyrae, which are exclu- ified version of figure taken from Jeffery & Saio (2016) sively old and metal-poor stars, have been used as stel- is shown. The line-shaded regions represent approximate lar tracers of the age, metallicity, extinction and struc- location of variables and the color represents approximate ture of our Galaxy but their use as robust distance in- spectral class mentioned on the top. The zero-age main dicators gained importance more recently thanks to the sequence (ZAMS) and the horizontal branch (ZAHB) are boost of near-infrared (NIR) observations over the last shown with solid and dashed red lines. Cepheid instability two decades. strip is shown with vertical black dashed lines. Dotted lines The goal of this review is to focus on recent represent evolutionary tracks of stars with different masses. progress on absolute calibration of classical Cepheids, The label on the left of the ZAMS shows the stellar mass of RR Lyrae and T2Cs, and their application to the each track. extragalactic distance scale. I strongly emphasize here that a short review can not fully describe all the aspects of these classical pulsating stars as standard 2006; Groenewegen & Jurkovic, 2017b; Jurkovic, 2018, and references therein) are not included in this candles. The interested readers are referred to the review. books, for example, Catelan & Smith (2015) on pul- This review is organised as follows: I describe sating variables and de Grijs (2011) on introduction briefly the description of evolutionary and pulsational to the cosmic distance scale. Additionally, several scenario for classical pulsating stars in Section 2 and excellent reviews are also available in the literature their light curve variations in Section 3. The Sections 4 (Madore & Freedman, 1991; Feast, 1999; Wallerstein, to 6 focus on classical Cepheids, RR Lyrae and T2Cs 2002; Sandage & Tammann, 2006; Catelan, 2009; as distance indicators both from the observational and Feast, 2013; Subramanian et al., 2017; Beaton et al., 2018, and references within). McWilliam (2011) theoretical perspectives at multiple wavelengths. The absolute scale for each standard candle and associated published an excellent set of online conference review systematics is also addressed. Finally, summary with articles on RR Lyrae stars focussed on different aspects an outlook for the future will be briefly presented in beyond their use as distance indicators while a recent Section 7. review of Cepheid and RR Lyrae as young and old stellar population tracers of the Galactic structure can be found in Matsunaga et al. (2018) and Kunder et al. 2. Evolutionary and Pulsational Scenario (2018), respectively. Note that while classical and T2Cs will be discussed extensively here, Anomalous Cepheid and RR Lyrae represent radially pulsating Cepheids (see, Wallerstein, 2002; Fiorentino et al., class of variable stars. Classical Cepheids are young J. Astrophys. Astr. (0000)000: #### Page 3 of 1 #### ( 10-300 Myr), intermediate-mass ( 3-10M ), metal- ⊙ 12 rich∼ stars while RR Lyrae are old ( 10∼ Gyr), low-mass ( 0.5-0.8M ) metal-poor stars. T2Cs≥ also belong to LMC CEP ∼ ⊙ RRL old, low-mass, metal-poor stellar populations. Clas- T2C sical pulsating variables populate a well-defined nar- row vertical region in temperature in the Hertzsprung- Russell (HR) diagram, known as the instability strip (IS). Fig. 1 shows the location of classical pulsat- 14 ing stars including Cepheid and RR Lyrae within the IS in the HR diagram. Classical Cepheids, repre- sented by the prototype δ Cep, are luminous yellow giant variables that pulsate in fundamental (FU), first- overtone (FO), second-overtone harmonics and multi- periodic (double/triple) modes (Soszyński et al., 2015). RR Lyrae occupy the region between the cross-section I 16 of the Horizontal Branch (HB) and the IS. Although RR Lyrae stars also pulsate primarily in the fundamental- mode (RRab) and first-overtone modes (RRc), few variables pulsating in more than one mode simultane- ously (RRd) have also been discovered (for example, Soszyński et al., 2017b). 18 The T2Cs represent different evolutionary states from post HB to the asymptotic giant branch (AGB) phase and a preliminary classification is done based on their pulsation periods: BL Herculis (BL Her, 1 . P . 4 d), W Virginis (W Vir, 4 . P . 20 d) and RV Tauri (RV Tau, P & 20 d). Soszyński et al. (2008) sug- 20 gested another subtype, peculiar W Virginis (pW Vir, 4 . P . 10 d), with distinct light curves and these 0 1 2 peculiar stars are mostly brighter and bluer than W V-I Vir. T2Cs primarily pulsate in the fundamental mode but BL Hers pulsating in the first-overtone mode have Figure 2.

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